Small scale structure in local interstellar matter (LISM) is considere
d. Overall morphology of the local cloud complex is inferred from Ca I
I absorption lines and observations of H I in white dwarf stars. Cloud
s with column densities ranging from 2-100 x 10(17) cm(-2) are found w
ithin 20 pc of the Sun. Cold (50 K) dense (similar to 10(5) cm(-3)) sm
all (5-10 au) clouds could be embedded and currently undetected in the
upwind gas. The Sun appears to be embedded in a filament of gas with
thickness less than or equal to 0.7 pc, and cross-wise column density
less than or equal to 2 x 10(17) cm(-2). The local magnetic field dire
ction is parallel to the filament, suggesting that the physical proces
s causing the filamentation is MHD related. Enhanced abundances of ref
ractory elements and LISM kinematics indicate outflowing gas from the
Scorpius-Centaurus Association. The local flow vector and lambda Sco d
ata are consistent with a 4,000,000 year old superbubble shell at simi
lar to-22 km s(-1), which is a shock front passing through preshock ga
s at similar to-12 km s(-1), and yielding cooled postshock gas at simi
lar to-26 km s(-1)in the upwind direction. A preshock magnetic held st
rength of 1.6 mu G, and postshock field strength of 5.2 mu G embedded
in the superbubble shell, are consistent with the data.